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Project Phoenix: the Australian deployment

机译：Project Phoenix：澳大利亚部署

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From February 2 until June 6 of 1995, the Phoenix Team conducted SETI observations using the 64 m radio telescope at Parkes and a remotely operated 22 m antenna at Connabarabran. The dual polarization observations covered the frequency range from 1.2 to 3 GHz using a single wideband receiver and two feeds built by CSIRO to support this project. The two antennas simultaneously observed a target list of 202 solar-type stars located at declinations south of $MIN@35 degrees. Individual observations lasted up to 276 seconds and examined 20 MHz of the spectrum with resolutions as fine as 1 Hz using hardware pattern detectors to search for narrowband, continuous or pulsed signals whose frequency might be slowly changing in time. The data were analyzed, and candidate signals were identified in near-real-time (before the end of the next data acquisition cycle). Those candidate signals not matched against an on-line RFI database were automatically reobserved with finer resolution by another set of detectors and followed in phase in order to permit a pseudo-interferometric measurement between the two telescopes. This two stage approach (detection on the 64 m antenna and immediate interferometric follow up of candidates) was part of a pipelined observational sequence and proved to be an extremely effective and efficient method of discriminating against RFI. Detection thresholds were set to produce a few candidate signals per observation, yet for more than 23,000 completed observations, the programmed sequence had to be interrupted fewer than 100 times to move the antennas off source for further verification procedures. In each case the candidate signals were found to be of our own technological making. The Phoenix observations in Australia failed to detect any ETI signals, but they also left no mysterious or unexplained signals hanging around. The deployment was a logistical and technological success, and reaffirms our opinion that one telescope is not enough.
机译：从2月2日到1995年6月6日，凤凰城队在帕克斯的64米广播望远镜进行了Seti观察，并在Connabarabran的一个远程操作的22米天线。双偏振观测使用单个宽带接收器和CSIRO构建的两个馈线覆盖了1.2到3 GHz的频率范围，以支持该项目。两个天线同时观察到了位于$ MIN @ 35度以南的拒绝的202型太阳能恒星的目标列表。个别观察持续最多276秒，并使用硬件模式检测器检验为1Hz的分辨率为20MHz，以搜索窄带，连续或脉冲信号，其频率可能会缓慢变化。分析数据，候选信号在接近实时（在下一个数据采集周期结束前）识别。与在线RFI数据库不匹配的那些候选信号被另一组探测器自动重新开始使用更精细的分辨率，并在阶段之后，以便允许两个望远镜之间的伪干涉测量测量。这两种阶段方法（检测64M天线和立即干涉候选者的候选者）是流水线观察序列的一部分，并被证明是一种极其有效和有效的鉴别RFI的方法。检测阈值设定为产生每观测几个候选信号，但对于超过23,000完成的观察，所述编程序列不得不被中断少于100倍来移动天线断源用于进一步的验证程序。在每种情况下，发现候选信号是我们自己的技术制作。澳大利亚的凤凰观测未能检测到任何ETI信号，但它们也没有悬挂的神秘或无法解释的信号。部署是一种后勤和技术成功，并重申我们认为一个望远镜还不够。

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